\section{Discussion}\label{Sec. Discussion}

 \subsection{Gas condition and dynamic characteristics}

     For all the cores,  $T_{12}/T_{13}$ range from 1.2 to 5.1 with average value of $2.2\pm0.8$, similar as that of \citet{wu2012gas}. Some spectra exhibit very small $T_{12}/T_{13}$ ratios, even equal strong emission for the two lines, such as spectrum of G159.21-20.12C1 ($T_{12}/T_{13}=1.18$ ), the flattening of \coa line is obvious. As the possibility of unsuitable reference point has been ruled out by the similarity of line profile as SMM 1 in \citet{2010ApJ...712..778H}, the cause of the flattening is still unknown.

     As non-gaussian line profiles may suggest remarkable dynamical feature, we investigate the deviation from Gaussian profile of our lines. The criteria are as the same as that in the paper by \citet{wu2012gas}.
     Within the \numcoretmc spectra of cores in TMC, 2 have blue profile and 1 of blue asymmetry; 4 have red profile and 2 have red asymmetry. In the only three cores in Perseus, 2 are found with blue profile and red profile, respectively. For CMC, five of the \numcorecmc cores show spectra with blue profile, while only one is with red profile. Two in the \numcorecmc cores in CMC are found with wings. The non-gaussian line profiles are presented as in Table \ref{LinePara}, column naming "Line Profile".

     Most of the cores that identified with wing(s) are found without obvious outflow configuration in the position-velocity(P-V) diagram, using method as \citet{2005AJ....129..330W}. Two cores (G164.75-24.19C2 and G173.07-17.89C1) exhibit convex isolines in their P-V diagrams, as shown in Figure \ref{Fig. PV_diagram}. G164.75-24.19C2 is supposed to be with outflow from the center of the core. While for G173.07-17.89C1, the convex part has a significant offset from the core, which may indicate the interaction between the core materials and the outer surrounding matters as well as the high-velocity turbulence accompanied. Generally, our samples of Planck clumps in the three regions are commonly without violent gas motions such as out-flows.


 \subsection{Coupling of gas and dust}

  \subsubsection{Excitation Temperature} \label{Sec. Gas-Dust coherent}

    Firstly we investigate the temperature coupling of the two major components of Planck cold clumps: gas and dust.
    We adopt the assumption of LTE, thus \texc of gas component derived from this work (see Section \ref{para_Tex}) is therefore can represent the kinetic temperature of the cores: $T_k$. While dust temperature are derived from \citet{2011yCat.8088....0P} column "TEMPERATURE\_CORE", denoted as $T_D$.

    We firstly use the core size given in ECC table (see \citet{2011yCat.8088....0P} i.e. the "MAJ\_AXIS\_FWHM\_CORE" ($\theta_{maj}$) and "MIN\_AXIS\_FWHM\_CORE")($\theta_{min}$) , and calculate the average gas \texc of our clumps within a circle with corresponding radius: $R=\sqrt{\pi\theta_{maj}\theta_{min}/[8\ln(2)]}$. The comparison of $T_K$ and $T_D$ is as shown in Figure \ref{Fig.Gas-Dust}.
    The $R^2$ of linear fitting of these $T_K$ and $T_D$ is as small as 0.001, indication relatively weak coherence of \texc between gas and dust component.

    Then we use the regions of "cores" defined by us i.e. we adopt the averaged \texc of our cores that have been calculated in Section \ref{Sec. Derived Parameters} to be compared with dust temperature, as shown in Figure \ref{Fig.Gas-Dust}.
    The correlation between $T_K$ and $T_D$ is still not obvious, indicated by $R^2\sim 10^{-5}$. Despite the poor correlation, we found that majority (61\%) of the cores have $T_D>T_K$, and with the $T_D/T_k$ of average value 1.3$\pm$0.4, which perhaps can be interpreted with the mechanism of gas heated by dust: Dust grains are heated by radiations from forming stellar objects in the center of the molecular clouds, and transfer energy to cooler gas by collisions( \citealt{1974ApJ...189..441G}).

  \subsubsection{CO abundance} \label{Sec. Gas-Dust coherent}

    To calculate the averaged column of our clumps in corresponding area as that in ECC, we also used the average in a circle with $R=\sqrt{\pi\theta_{maj}\theta_{min}/[8\ln(2)]}$ and got the $N_{^{12}\rm CO}$. For the dust component, we adopted the method adopted by \citet{2011A&A...536A..23P} and calculated the \nhyd via dust component. Thus, the CO abundance was calculated as $N_{^{12}\rm CO}/N_{H_2}$. For all the clumps, CO abundance ranges from $4\times 10^{-7}$ to$1.3\times 10^{-3}$
    average at $1.5\times 10^{-4}$, consistent with the variance obtained by \citet{1988ApJ...334..771V}.

    The spatia distribution of the CO abundance is plotted as Figure \ref{Fig.COAbundance}, from which we can notice that the cores near the center of the complex averagely have larger CO abundance.

  \subsection{Turbulence}\label{Sec. Velocity dispersion}

    Previous works often reveal turbulence are  subsonic in cores while supersonic in the whole cloud, and compared to thermal component, turbulent motions is a minor contribution to core supporting(\citealt{1983ApJ...270..105M}, \citealt{2004A&A...416..191T}). However, as shown in Figure \ref{Fig.SigmaTH/SigmaNT}, majority of cores in both TMC and CMC are of \sigmant /\sigmath$>1$ and the estimated ratio of non-thermal pressure to thermal pressure $R_p=\frac{\sigma^2_{NT}}{\sigma^2_{Therm}}$ is therefore generally larger than 1, revealing that these cores are mainly turbulence dominated.

    The dominance of turbulence indicate that the gravitational contracting or collapse is rare in our cores of both regions, otherwise the turbulence will soon decay on a dynamic timescale (\citealt{shu1987star}). This reflects that \Planck clumps in TMC and CMC are  also quiescent and not affected by gravity greatly. Especially for CMC, only one core is with \sigmath (0.23 km/s) larger than \sigmant (0.21 km/s), such an overwhelming dominance in CMC may reflect the inactivity of star formation therein.

 \subsection{Gravitational stabilities of the cores} \label{Sec. Gravitational stabilities of the cores}

    To calculate the $M_{LTE}$ we use the \nhyd calculated in Section \ref{Sec. Derived Parameters}, which are the averaged values within the ellipses described by the offsets and deconvolved sizes in Table \ref{core_properties}. Thus, $M_{LTE}$ can be calculated as:
    \begin{equation}
        M_{LTE}=\pi R^2 m_H \mu N_{H_2}
    \end{equation}
    $m_H$ is the mass of H atom and $\mu=2.33$ is the mean molecular weight.

    Assuming that the cores are gravitationally bound isothermal sphere with uniform density and is supported solely by random motions, the virial mass $M_{vir}$ can be calculated following \citet{2000ApJ...537..221U}:

    \begin{equation}
        \frac{M_{vir}}{M_\odot} = 2.10\times 10^{2}\left(\frac{R}{\rm pc}\right)\left(\frac{\Delta V}{\rm km\ s^{-1}}\right)^2
    \end{equation}

    where R is the radius of the core and $\Delta V $ is the FWHM of \cob (if there is no \coc detection) or FWHM of \coc. Thus we can test that if the cores are bound by comparing the $M_{vir}$ with there $M_{LTE}$.

    In molecular clouds, many factors including thermal pressure, turbulence, and magnetic field can support the gas against self gravity. Taking thermal and turbulent motion support into account, the Jeans Mass $M_{J}$ of each core was calculated as following(Hennebelle \& Chabrier 2008):

    \begin{equation}
        \frac{M_{J}}{M_\odot} \approx 1.0a_J \left(\frac{T_{eff}}{10 \rm K}\right)  ^{3/2}  \left(\frac{\mu}{2.33}\right) ^{-1/2} \left(\frac{n}{10^4\ \rm cm^{-3}}\right)^{-1/2}
    \end{equation}

    where $a_J$ is a dimensionless parameter of order unity which takes into account of the geometrical factor, $\mu =2.33$ is the mean molecular weight, $n$ is the volume density of H$_2$. The effective temperature $T_{eff}$ is :

    \begin{equation}
        T_{eff} = \frac{C^2_{s, eff} \mu m_{H}}{k}
    \end{equation}
    and the effective sound ($C_{s, eff}$) speed is:
    \begin{equation}
      C_{s, eff}= (\sigma ^2 _{NT}+\sigma ^2 _{Therm})^{1/2}
    \end{equation}


    For the cores in both TMC and CMC, the $M_{LTE}$, $M_{vir}$ and $M_{J}$ were compared with each other, shown as Figure \ref{mass_tmc} and Figure \ref{mass_cmc}. One can see that 17 of the 19 cores in TMC are with $M_J$ larger than $M_{LTE}$, which suggest that the cores are probably without gravitational collapsing. For 16 cores in CMC, 10 cores are with $M_J$ larger than $M_{LTE}$, of the rest 6 cores with $M_{LTE}>M_J$, three (G156.92-09.72C1, G157.12-11.56C1, G157.60-12.17bC1) are of blue profile spectra, which may be hint of gravitational collapse. Remarkably, G157.60-12.17bC1 is the only one in CMC that has \sigmath $>$ \sigmant, which suggests an additional hint of gravitational collapse.
    Despite these, we still cannot ignore the limitation of our resolution. In the distance of CMC (450 pc), the beam size of our observation is equivalent to $\sim 0.1$ pc, which may cannot resolve the cores with that with typical size range of $0.03~0.2$ pc (\citealt{2007ARA&A..45..339B}). Thus, we may have overestimated the sizes of the cores and as $M_{vir}\propto R$ and $M_{vir}\propto R^{1/2}$ while $M_{LTE}\propto R^2$, the $M_{LTE}$ may be more overestimated than they other two and thus exceed them.

    Meanwhile, all of the cores are with $M_{vir}>M_{LTE}$. The mean virial ratio $\alpha=\frac{M_{vir}}{M_{LTE}}$ of cores in TMC is 51, with large standard deviation of 58. Only four cores in TMC are with LTE ratio less than 3, and 63\% of the cores are with LTE ratio larger than 10.
    For the 16 cores in CMC, the LTE ratio is with average value of $9\pm6$ and 13 cores are found with LTE ratio exceed 3.
    Such large $\alpha$ indicate that they are not bound and may be dynamically evolving, in a transient state.


 \subsection{Associated objects of mapped regions}

    To further investigate the conditions and environment of the mapped clumps, we examined their associate objects. The mapped field of $14\arcmin\times 14\arcmin$ has been checked. Objects included are X-ray object, radio, \textsc{H i}, Maser, IR object, HH object and YSO.
    The associated objects are as shown in Figure \ref{Maps}.

    To ensure a fair comparison, we also checked the Spitzer YSO survey coverage of each source: If a source is of IRAC \emph{or} MIPS observation (\citealt{2010ApJS..186..259R}) within its mapping region, it will be regarded as covered by Spitzer YSO, and denoted "Y" in Table \ref{sources}, otherwise, it will be regarded as uncovered and denoted "N". As the survey done by \citep{2013ApJ...764..133H} provides us a ideal catalogue of YSO in CMC, we also checked the association of our sources with the two catalogs of this study.

    Among the \numsoucmc clumps in CMC, G159.82-10.48 and G160.53-09.84 are found with X-ray object(s). Six clumps are found with radio, H I or Maser sources, while nine are found with IR objects. Two clumps: G155.52-08.93 and G160.53-09.84 are found with HH object. From the CMC survey by \citep{2013ApJ...764..133H}, we found only 4 clumps are associated with YSO.
    Such a rare association with YSO may indicate the low activity of star formation, which is consistent with previous researches.

    In TMC, a more active environment is revealed by the association analysis. Among the \numsoutmc clumps, 13 are found associated with X-ray source, 14 are found with radio, H I or Maser, while as much as 16 are found with IR objects. HH objects were found in 8 of them. In Taurus, Spitzer IRAC \emph{or} MIPS were found cover 28 clumps, while only in 8 of them, YSO were found.

    PMC is much more active and abundant of associated objects: Although there are only \numsoupmc clumps in our sample, 2 of them are with x-ray sources, while 7 of them are radio, H I or Maser sources. 8 are found with IR objects and 7 with HH objects. YSO are found in 6 of them. Not only most of the clumps are found with associated objects, the abundance of the associated objects is also considerable, such as G158.20-20.28 and G158.37-20.72. Remarkably, we found that G159.21-20.12 is a part of dark cloud Barnard 1 (\citealt{1986ApJ...303L..11G}) and G160.51-17.07 is a part of Barnard 5 (\citealt{2010ApJ...712..778H}). Additionally, G159.21-20.12 shows a \coaa spectrum that resemble that of SMM 1 in \citep{2010ApJ...712..778H}.

    Most of the cores are without associated objects in the confine of circle of radius as same as beam size ($\sim$ 1 arc min) at there centers. The few exceptions are the cores that are with larger spatial extension. Such as for G159.21-20.12C1, several young stellar objects (YSO) and candidate YSO and HH objects were found associated, and this is also the largest and most massive core in our samples and is rather diffuse than other cores. Similarly, as a core of large size, G174.70-15.48C1 is also found with YSO, X-ray source, and infrared source (IR) in its densest part. Besides them,  G164.75-24.19C2 and G164.92-12.65C1 are both found with IR in their centers.  For other dense cores, the associated objects, if any, are often surrounding the cores in the outer parts, such as G159.82-10.48C1, and more are without any associated objects found in the mapped areas. Thus, despite that 70 \% of the cores are found with associated objects mentioned above, 34 of \numcore  cores are without associated objects within their center parts, suggesting that they are sourceless.

    Remarkably, for the three cores with associated sources in TMC: G164.75-24.19C2 and G164.92-12.65C1 are both with \sigmath larger than \sigmant, which is a suggestion of more mature stage of evolution as discussed in Section \ref{Sec. Velocity dispersion}. G174.70-15.48C1 is with \texc of 14.0 K, which is the highest among the cores in TMC, also indication a later revolutionary stage.

